Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron
The radio and gamma-ray pulsar PSR J2032+4127 was recently found to be in a decades-long orbit with the Be star MT91 213, with the pulsar moving rapidly towards periastron. This binary shares many similar characteristics with the previously unique binary system PSR B1259-63/LS 2883. Here in this pap...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2016-09, Vol.464 (1) |
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| container_title | Monthly notices of the Royal Astronomical Society |
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| creator | Ho, Wynn C. G. Ng, C. -Y. Lyne, Andrew G. Stappers, Ben W. Coe, Malcolm J. Halpern, Jules P. Johnson, Tyrel J. Steele, Iain A. |
| description | The radio and gamma-ray pulsar PSR J2032+4127 was recently found to be in a decades-long orbit with the Be star MT91 213, with the pulsar moving rapidly towards periastron. This binary shares many similar characteristics with the previously unique binary system PSR B1259-63/LS 2883. Here in this paper, we describe radio, X-ray, and optical monitoring of PSR J2032+4127/MT91 213. Our extended orbital phase coverage in radio, supplemented with Fermi LAT gamma-ray data, allows us to update and refine the orbital period to 45–50 yr and time of periastron passage to 2017 November. We analyse archival and recent Chandra and Swift observations and show that PSR J2032+4127/MT91 213 is now brighter in X-rays by a factor of ~70 since 2002 and ~20 since 2010. While the pulsar is still far from periastron, this increase in X-rays is possibly due to collisions between pulsar and Be star winds. Optical observations of the Hα emission line of the Be star suggest that the size of its circumstellar disc may be varying by ~2 over time-scales as short as 1–2 months. In conclusion, multiwavelength monitoring of PSR J2032+4127/MT91 213 will continue through periastron passage, and the system should present an interesting test case and comparison to PSR B1259-63/LS 2883. |
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G. ; Ng, C. -Y. ; Lyne, Andrew G. ; Stappers, Ben W. ; Coe, Malcolm J. ; Halpern, Jules P. ; Johnson, Tyrel J. ; Steele, Iain A.</creator><creatorcontrib>Ho, Wynn C. G. ; Ng, C. -Y. ; Lyne, Andrew G. ; Stappers, Ben W. ; Coe, Malcolm J. ; Halpern, Jules P. ; Johnson, Tyrel J. ; Steele, Iain A. ; SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)</creatorcontrib><description>The radio and gamma-ray pulsar PSR J2032+4127 was recently found to be in a decades-long orbit with the Be star MT91 213, with the pulsar moving rapidly towards periastron. This binary shares many similar characteristics with the previously unique binary system PSR B1259-63/LS 2883. Here in this paper, we describe radio, X-ray, and optical monitoring of PSR J2032+4127/MT91 213. Our extended orbital phase coverage in radio, supplemented with Fermi LAT gamma-ray data, allows us to update and refine the orbital period to 45–50 yr and time of periastron passage to 2017 November. We analyse archival and recent Chandra and Swift observations and show that PSR J2032+4127/MT91 213 is now brighter in X-rays by a factor of ~70 since 2002 and ~20 since 2010. While the pulsar is still far from periastron, this increase in X-rays is possibly due to collisions between pulsar and Be star winds. Optical observations of the Hα emission line of the Be star suggest that the size of its circumstellar disc may be varying by ~2 over time-scales as short as 1–2 months. In conclusion, multiwavelength monitoring of PSR J2032+4127/MT91 213 will continue through periastron passage, and the system should present an interesting test case and comparison to PSR B1259-63/LS 2883.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><language>eng</language><publisher>United States: Royal Astronomical Society</publisher><subject>ASTRONOMY AND ASTROPHYSICS ; binaries ; emission line ; individual ; MT91 213 ; neutron ; PSR B1259−63 ; PSR J2032+4127 ; pulsars ; stars ; X-rays</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2016-09, Vol.464 (1)</ispartof><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881</link.rule.ids><backlink>$$Uhttps://www.osti.gov/servlets/purl/1355747$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Ho, Wynn C. G.</creatorcontrib><creatorcontrib>Ng, C. -Y.</creatorcontrib><creatorcontrib>Lyne, Andrew G.</creatorcontrib><creatorcontrib>Stappers, Ben W.</creatorcontrib><creatorcontrib>Coe, Malcolm J.</creatorcontrib><creatorcontrib>Halpern, Jules P.</creatorcontrib><creatorcontrib>Johnson, Tyrel J.</creatorcontrib><creatorcontrib>Steele, Iain A.</creatorcontrib><creatorcontrib>SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)</creatorcontrib><title>Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron</title><title>Monthly notices of the Royal Astronomical Society</title><description>The radio and gamma-ray pulsar PSR J2032+4127 was recently found to be in a decades-long orbit with the Be star MT91 213, with the pulsar moving rapidly towards periastron. This binary shares many similar characteristics with the previously unique binary system PSR B1259-63/LS 2883. Here in this paper, we describe radio, X-ray, and optical monitoring of PSR J2032+4127/MT91 213. Our extended orbital phase coverage in radio, supplemented with Fermi LAT gamma-ray data, allows us to update and refine the orbital period to 45–50 yr and time of periastron passage to 2017 November. We analyse archival and recent Chandra and Swift observations and show that PSR J2032+4127/MT91 213 is now brighter in X-rays by a factor of ~70 since 2002 and ~20 since 2010. While the pulsar is still far from periastron, this increase in X-rays is possibly due to collisions between pulsar and Be star winds. Optical observations of the Hα emission line of the Be star suggest that the size of its circumstellar disc may be varying by ~2 over time-scales as short as 1–2 months. In conclusion, multiwavelength monitoring of PSR J2032+4127/MT91 213 will continue through periastron passage, and the system should present an interesting test case and comparison to PSR B1259-63/LS 2883.</description><subject>ASTRONOMY AND ASTROPHYSICS</subject><subject>binaries</subject><subject>emission line</subject><subject>individual</subject><subject>MT91 213</subject><subject>neutron</subject><subject>PSR B1259−63</subject><subject>PSR J2032+4127</subject><subject>pulsars</subject><subject>stars</subject><subject>X-rays</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2016</creationdate><recordtype>article</recordtype><recordid>eNqNyktKA0EQgOEmKDhG71C4lcF-zMNsFUWEgGgW2YVOpzNTYawaukslnsazeDIJ6N7VDx__RBXGNXVpZ01zpAqtXV1et8acqNOcd1rrytmmUJ_zt0Hww7_HIVInPbwyoXBC6sDTBpZl8ntYJ-x6iXRQ3sJN_HMkn_bw9PIMj1Y7e1kZ217NFzPz_WWNAyZAyeDHMbEPPQjDGBP6LInpTB1v_ZDj-W-n6uL-bnH7UHIWXOWAEkMfmCgGWRlX123Vun9NP3XzTTQ</recordid><startdate>20160922</startdate><enddate>20160922</enddate><creator>Ho, Wynn C. G.</creator><creator>Ng, C. -Y.</creator><creator>Lyne, Andrew G.</creator><creator>Stappers, Ben W.</creator><creator>Coe, Malcolm J.</creator><creator>Halpern, Jules P.</creator><creator>Johnson, Tyrel J.</creator><creator>Steele, Iain A.</creator><general>Royal Astronomical Society</general><scope>OIOZB</scope><scope>OTOTI</scope></search><sort><creationdate>20160922</creationdate><title>Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron</title><author>Ho, Wynn C. G. ; Ng, C. -Y. ; Lyne, Andrew G. ; Stappers, Ben W. ; Coe, Malcolm J. ; Halpern, Jules P. ; Johnson, Tyrel J. ; Steele, Iain A.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-osti_scitechconnect_13557473</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2016</creationdate><topic>ASTRONOMY AND ASTROPHYSICS</topic><topic>binaries</topic><topic>emission line</topic><topic>individual</topic><topic>MT91 213</topic><topic>neutron</topic><topic>PSR B1259−63</topic><topic>PSR J2032+4127</topic><topic>pulsars</topic><topic>stars</topic><topic>X-rays</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Ho, Wynn C. G.</creatorcontrib><creatorcontrib>Ng, C. -Y.</creatorcontrib><creatorcontrib>Lyne, Andrew G.</creatorcontrib><creatorcontrib>Stappers, Ben W.</creatorcontrib><creatorcontrib>Coe, Malcolm J.</creatorcontrib><creatorcontrib>Halpern, Jules P.</creatorcontrib><creatorcontrib>Johnson, Tyrel J.</creatorcontrib><creatorcontrib>Steele, Iain A.</creatorcontrib><creatorcontrib>SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)</creatorcontrib><collection>OSTI.GOV - Hybrid</collection><collection>OSTI.GOV</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Ho, Wynn C. G.</au><au>Ng, C. -Y.</au><au>Lyne, Andrew G.</au><au>Stappers, Ben W.</au><au>Coe, Malcolm J.</au><au>Halpern, Jules P.</au><au>Johnson, Tyrel J.</au><au>Steele, Iain A.</au><aucorp>SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2016-09-22</date><risdate>2016</risdate><volume>464</volume><issue>1</issue><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>The radio and gamma-ray pulsar PSR J2032+4127 was recently found to be in a decades-long orbit with the Be star MT91 213, with the pulsar moving rapidly towards periastron. This binary shares many similar characteristics with the previously unique binary system PSR B1259-63/LS 2883. Here in this paper, we describe radio, X-ray, and optical monitoring of PSR J2032+4127/MT91 213. Our extended orbital phase coverage in radio, supplemented with Fermi LAT gamma-ray data, allows us to update and refine the orbital period to 45–50 yr and time of periastron passage to 2017 November. We analyse archival and recent Chandra and Swift observations and show that PSR J2032+4127/MT91 213 is now brighter in X-rays by a factor of ~70 since 2002 and ~20 since 2010. While the pulsar is still far from periastron, this increase in X-rays is possibly due to collisions between pulsar and Be star winds. Optical observations of the Hα emission line of the Be star suggest that the size of its circumstellar disc may be varying by ~2 over time-scales as short as 1–2 months. In conclusion, multiwavelength monitoring of PSR J2032+4127/MT91 213 will continue through periastron passage, and the system should present an interesting test case and comparison to PSR B1259-63/LS 2883.</abstract><cop>United States</cop><pub>Royal Astronomical Society</pub><oa>free_for_read</oa></addata></record> |
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| subjects | ASTRONOMY AND ASTROPHYSICS binaries emission line individual MT91 213 neutron PSR B1259−63 PSR J2032+4127 pulsars stars X-rays |
| title | Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron |
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